The accretion luminosity (\(L_{\text{\,acc}}\) ) of a young star is produced by the shocked material falling onto the stellar photosphere. The accretion energy released is seen in the form of continuum excess in emission – mostly at ultraviolet (UV) and optical wavelengths – and emission lines. Historically, the \(L_{\text{\,acc}}\)  of low-mass young stars is estimated by modelling the Paschen and Balmer continua emission as isothermal slabs [1]}, [2]}. More often, \(L_{\text{\,acc}}\)  has been computed from empirical relations
between the luminosity of accretion-tracing lines and \(L_{\text{\,acc}}\)  [3]}, [4]}, [5]}.
[6]} derived more precise relationships between the line luminosity (\(L_{\,\text{line}}\) ) of several optical and near-infrared (NIR) accretion-tracing emission lines and \(L_{\text{\,acc}}\) .
